Swift and Chandra Detections of Supernova 2006jc: Evidence for Interaction of the Supernova Shock with a Circumstellar Shell

TL;DR

This study reports Swift and Chandra observations of supernova 2006jc, revealing shock interaction with a dense circumstellar shell formed by progenitor mass ejection, providing insights into pre-supernova stellar behavior.

Contribution

It presents the first combined UV and X-ray observational evidence of shock interaction with a circumstellar shell in supernova 2006jc, linking it to progenitor mass ejection episodes.

Findings

X-ray emission increased by a factor of ~5 over 4 months

Detection of MgII 2800A line emission in UV spectra

Evidence of a dense shell at ~16 cm from explosion site

Abstract

The peculiar Type Ib supernova (SN) 2006jc has been observed with the UV/Optical Telescope (UVOT) and X-Ray Telescope (XRT) on board the Swift observatory over a period of 19 to 183 days after the explosion. Signatures of interaction of the outgoing SN shock with dense circumstellar material (CSM) are detected, such as strong X-ray emission (L_{0.2-10} > E39 erg/s) and the presence of MgII 2800A line emission visible in the UV spectra. In combination with a Chandra observation obtained on day 40 after the explosion, the X-ray light curve is constructed, which shows a unique rise of the X-ray emission by a factor of ~5 over a period of ~4 months, followed by a rapid decline. We interpret the unique X-ray and UV properties as a result of the SN shock interacting with a shell of material that was deposited by an outburst of the SN progenitor two years prior to the explosion. Our results are consistent with the explosion of a Wolf-Rayet star that underwent an episodic mass ejection qualitatively similar to those of luminous blue variable stars prior to its explosion. This led to the formation of a dense (>E7 cm**-3) shell at a distance of ~E16 cm from the site of the explosion, which expands with the WR wind at a velocity of (1300+/-300) km/s.